A. M. Tatarnikov
Moscow State University
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Featured researches published by A. M. Tatarnikov.
Proceedings of SPIE | 2014
Vladimir Ya. Molchanov; Sergey P. Anikin; Sergey I. Chizhikov; Konstantin B. Yushkov; Oleg Makarov; A. M. Tatarnikov; S. A. Potanin; Valentin F. Esipov
We report design and prototype performance of an acousto-optical imaging spectropolarimeter aimed for the 2.5 m telescope at Caucasian Mountain Observatory of Lomonosov Moscow State University. Special geometry of the acousto-optical interaction provides two diffracted beams polarized along the slow and the fast axes of the crystal. The optical system of the spectrometer consisting of plane and elliptical mirrors delivers the images of the object with two orthogonal polarizations to a single CCD matrix, increasing the focal ratio of the telescope.
Monthly Notices of the Royal Astronomical Society | 2017
V.L. Oknyansky; C.M. Gaskell; N.A. Huseynov; V. Lipunov; N. I. Shatsky; Sergey S. Tsygankov; E. Gorbovskoy; K.M. Mikailov; A. M. Tatarnikov; D.A. Buckley; V.G. Metlov; A. E. Nadzhip; A. Kuznetsov; P.V. Balanutza; Burlak; G.A. Galazutdinov; B. P. Artamonov; I.R. Salmanov; Konstantin Malanchev; R.S. Oknyansky
Optical and near-infrared photometry, optical spectroscopy, and soft X-ray and UV monitoring of the changing look active galactic nucleus NGC 2617 show that it continues to have the appearance of a type-1 Seyfert galaxy. An optical light curve for 2010-2016 indicates that the change of type probably occurred between 2010 October and 2012 February and was not related to the brightening in 2013. In 2016 NGC 2617 brightened again to a level of activity close to that in 2013 April. We find variations in all passbands and in both the intensities and profiles of the broad Balmer lines. A new displaced emission peak has appeared in H
Astronomy Reports | 2009
A. A. Tatarnikova; A. M. Tatarnikov
\beta
Astronomy Letters | 2001
A.E. Nadzhip; A. M. Tatarnikov; V. I. Shenavrin; G. Weigelt; B. F. Yudin
. X-ray variations are well correlated with UV-optical variability and possibly lead by
Astronomy Letters | 2000
V. F. Esipov; E. A. Kolotilov; J. Mikolajewska; Ulisse Munari; A. A. Tatarnikova; A. M. Tatarnikov; T. Tomov; B. F. Yudin
\sim
Astronomy Letters | 2014
O. G. Taranova; A. M. Tatarnikov; V. I. Shenavrin; A. A. Tatarnikova
2-3 d. The
Astronomy Reports | 2011
A. A. Tatarnikova; A. M. Tatarnikov; V. F. Esipov; T.N. Tarasova; V. I. Shenavrin; E. A. Kolotilov; A. E. Nadzhip
K
Astronomy Letters | 2009
A. A. Tatarnikova; A. M. Tatarnikov; V. F. Esipov; E. A. Kolotilov
band lags the
Astronomy Letters | 2009
O. G. Taranova; V. I. Shenavrin; A. M. Tatarnikov
J
Optics and Spectroscopy | 2016
Sergey P. Anikin; V. F. Esipov; V.Ya. Molchanov; A. M. Tatarnikov; K. B. Yushkov
band by about 21.5
